2012/11/30 by Jim Fuller, Dong Lai · 57 citations
Physics and Astronomy · #Amplitude #Astro and Planetary Science #Astrophysics #Gamma-ray bursts and supernovae #Luminosity #Orbital period #Physics #Rotation period #Stars #Stellar, planetary, and galactic studies #Surface gravity #Tidal heating #White dwarf #astro-ph.HE #astro-ph.SR
paper · pdf · doi:10.1093/mnras/sts606
published in Monthly Notices of the Royal Astronomical Society 430(1), 274-287 (Oxford University Press) · 23 pages, 12 figures, accepted to MNRAS
arxiv created 2012/12/18 · openalex publication_date 2013/01/25 · arxiv updated 2015/06/12 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Tidal dissipation in compact white dwarf (WD) binary systems significantly influences the physical conditions (such as surface temperature and rotation rate) of the WDs prior to mass transfer or merger. In these systems, the dominant tidal effects involve the excitation of gravity waves and their dissipation in the outer envelope of the star. We calculate the amplitude of tidally excited gravity waves in low-mass (0.3 M⊙) helium (He) core WDs as a function of the tidal forcing frequency ω. Like carbon–oxygen (CO) WDs studied in our previous paper, we find that the dimensionless tidal torque F(ω) (inversely proportional to the effective tidal quality factor) depends on ω in an erratic way. On average, F(ω) scales approximately as ω6, and is several orders of magnitude smaller for He WDs than for CO WDs. We find that tidal torques can begin to synchronize the WD rotation when the orbital period is less than about an hour, although a nearly constant asynchronization is maintained even at small periods. We examine where the tidally excited gravity waves experience non-linear breaking or resonant absorption at a critical layer, allowing us to estimate the location and magnitude of tidal heating in the WD envelope. We then incorporate tidal heating in the mesa stellar evolution code, calculating the physical conditions of the WD as a function of orbital period for different WD models. We find that tidal heating makes a significant contribution to the WD luminosity for short-period (∼10 min) systems such as SDSS J0651+2844. We also find that for WDs containing a hydrogen envelope, tidal heating can trigger runaway hydrogen shell burning, leading to a nova-like event before the onset of mass transfer.